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Table 1

Source parameters.

Source RA Dec D νLSRa Lbolb Tbolb Menvc References
(h m s) (°′′′) (pc) (km s-1) (L⊙) (K) (M⊙)
L1448-MM 03 25 38.9  + 30 44 05.4 235  + 4.7 9.0 46 3.9 1, 2
NGC 1333-IRAS2A 03 28 55.6  + 31 14 37.1 235  + 7.7 35.7 50 5.1 1, 3
NGC 1333-IRAS4A 03 29 10.5  + 31 13 30.9 235  + 7.2 9.1 33 5.6 1, 3
NGC 1333-IRAS4B 03 29 12.0  + 31 13 08.1 235  + 7.4 4.4 28 3.0 1, 3
L1527 04 39 53.9  + 26 03 09.8 140  + 5.9 1.9 44 0.9 1, 3
Ced110-IRS4 11 06 47.0  −77 22 32.4 125  + 3.5 0.8 56 0.2 4, 5
BHR71 12 01 36.3  −65 08 53.0 200  −4.4 14.8 44 2.7 6, 7
IRAS 15398e 15 43 01.3  −34 09 15.0 130  + 5.1 1.6 52 0.5 4, 5
L483 18 17 29.9  −04 39 39.5 200  + 5.2 10.2 49 4.4 1, 8
Ser SMM1 18 29 49.8  + 01 15 20.5 230d  + 8.5 30.4 39 16.1 9, 10
Ser SMM4 18 29 56.6  + 01 13 15.1 230d  + 8.0 1.9 26 2.1 9, 10
Ser SMM3 18 29 59.2  + 01 14 00.3 230d  + 7.6 5.1 38 3.2 9, 10
L723 19 17 53.7  + 19 12 20.0 300  + 11.2 3.6 39 1.3 11, 12
B335 19 37 00.9  + 07 34 09.6 250  + 8.4 3.3 36 1.2 1, 13
L1157 20 39 06.3  + 68 02 15.8 325  + 2.6 4.7 46 1.5 1, 14
NGC 1333-IRAS3 03 29 03.8  + 31 16 04.0 235  + 8.5 41.8 149 9.5 15, 2
L1489 04 04 43.0  + 26 18 57.0 140  + 7.2 3.8 200 0.2 16, 17
L1551-IRS5 04 31 34.1  + 18 08 05.0 140  + 7.2 22.1 94 2.3 11,17
TMR1e 04 39 13.7  + 25 53 21.0 140  + 6.3 3.8 133 0.2 18, 17
TMC1Ae 04 39 34.9  + 25 41 45.0 140  + 6.6 2.7 118 0.2 18, 17
TMC1 04 41 12.4  + 25 46 36.0 140  + 5.2 0.9 101 0.2 18, 17
HH46-IRS 08 25 43.9  −51 00 36.0 450  + 5.2 27.9 104 4.4 19, 20
IRAS 12496 12 53 17.2  −77 07 10.6 178  + 2.3 35.4 569 0.8 4, 21
GSS30-IRS1 16 26 21.4  −24 23 04.0 125  + 2.8 13.9 142 0.1 22, 23
Elias 29 16 27 09.4  −24 37 19.6 125  + 5.0 14.1 299 0.04 24, 23
Oph-IRS63 16 31 35.6  −24 01 29.6 125  + 2.8 1.0 327 0.3 24, 23
RNO91 16 34 29.3  −15 47 01.4 125  + 5.0 2.6 340 0.5 4, 23
RCrA-IRS5A 19 01 48.0  −36 57 21.6 130  + 5.7 7.1 126 2.0 4, 5
HH100-IRS 19 01 49.1  −36 58 16.0 130  + 5.6 17.7 256 8.1 4, 5

Notes. Sources above the horizontal line are Class 0, sources below are Class I.

(a)

Obtained from ground-based C18O or C17O observations.

(b)

Measured using Herschel-PACS data from the WISH and DIGIT key programmes (Karska et al., in prep.; Green et al., in prep.).

(c)

Determined from DUSTY modelling of the sources; see Appendix C.

(d)

Using VLBA observations of a star thought to be associated with the Serpens cluster, Dzib et al. (2010) derive a distance of 415 pc.

(e)

The coordinates used in WISH; more accurate SMA coordinates of the sources are 15h43m022,  − 34°09′068 (IRAS 15398), 04h39m139,  + 25°53′206 (TMR1) and 04h39m352,  + 25°41′444 (TMC1A; Jørgensen et al. 2009).

References. (1) Jørgensen et al. (2007); (2) Hirota et al. (2011); (3) Hirota et al. (2008); (4) Evans et al. (2009); (5) Knude & Høg (1998); (6) Chen et al. (2008); (7) Seidensticker & Schmidt-Kaler (1989); (8) Fuller et al. (1995); (9) Hogerheijde et al. (1999); (10) Eiroa et al. (2008); (11) Jørgensen et al. (2002); (12) Goldsmith & Sernyak (1984); (13) Frerking et al. (1987); (14) Straizys et al. (1992); (15) Bachiller et al. (1998); (16) Brinch et al. (2007); (17) Kenyon et al. (2008); (18) Hogerheijde et al. (1998); (19) Velusamy et al. (2007); (20) Noriega-Crespo et al. (2004); (21) Whittet et al. (1997); (22) Jørgensen et al. (2009); (23) de Geus et al. (1989); (24) Lommen et al. (2008).

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